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  Magnetizing the circumgalactic medium of disc galaxies

Pakmor, R., van de Voort, F., Bieri, R., Gómez, J. M., Grand, R. J. J., Guillet, T., et al. (2020). Magnetizing the circumgalactic medium of disc galaxies. Monthly Notices of the Royal Astronomical Society, 498(3), 3125-3137. doi:10.1093/mnras/staa2530.

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 Creators:
Pakmor, Rüdiger1, Author              
van de Voort, Freeke2, Author              
Bieri, Rebekka3, Author              
Gómez, José Manuel, Author
Grand, Robert J. J.2, Author              
Guillet, Thomas, Author
Marinacci, Federico, Author
Pfrommer, Christoph, Author
Simpson, Christine M., Author
Springel, Volker4, Author              
Affiliations:
1Stellar Astrophysics, MPI for Astrophysics, Max Planck Society, ou_159882              
2Galaxy Formation, Cosmology, MPI for Astrophysics, Max Planck Society, ou_159878              
3Galaxy Formation, MPI for Astrophysics, Max Planck Society, ou_2205643              
4Computational Structure Formation, MPI for Astrophysics, Max Planck Society, ou_2205642              

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 Abstract: The circumgalactic medium (CGM) is one of the frontiers of galaxy formation and intimately connected to the galaxy via accretion of gas on to the galaxy and gaseous outflows from the galaxy. Here, we analyse the magnetic field in the CGM of the Milky Way-like galaxies simulated as part of the auriga project that constitutes a set of high-resolution cosmological magnetohydrodynamical zoom simulations. We show that before z = 1 the CGM becomes magnetized via galactic outflows that transport magnetized gas from the disc into the halo. At this time, the magnetization of the CGM closely follows its metal enrichment. We then show that at low redshift an in situ turbulent dynamo that operates on a time-scale of Gigayears further amplifies the magnetic field in the CGM and saturates before z = 0. The magnetic field strength reaches a typical value of 0.1μG at the virial radius at z = 0 and becomes mostly uniform within the virial radius. Its Faraday rotation signal is in excellent agreement with recent observations. For most of its evolution, the magnetic field in the CGM is an unordered small-scale field. Only strong coherent outflows at low redshift are able to order the magnetic field in parts of the CGM that are directly displaced by these outflows.

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 Dates: 2020-08-21
 Publication Status: Published online
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 Rev. Type: Peer
 Identifiers: DOI: 10.1093/mnras/staa2530
Other: LOCALID: 3281087
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Title: Monthly Notices of the Royal Astronomical Society
  Other : Mon. Not. R. Astron. Soc.
Source Genre: Journal
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Publ. Info: Oxford : Oxford University Press
Pages: - Volume / Issue: 498 (3) Sequence Number: - Start / End Page: 3125 - 3137 Identifier: ISSN: 1365-8711
CoNE: https://pure.mpg.de/cone/journals/resource/1000000000024150